The improvements in the stellar and supernova nucleosynthesis theory and modelization [1]}, [2]} established that the major astrophysical sources of the chemical elements are: i) Core-collapse supernovae (SNcc) and their massive progenitors (\(\gtrsim 8-10 M_\odot \) ) synthesise most of the O, Ne, and Mg of the Universe and a considerable fraction of Si and S (collectively called \(\alpha \)  elements as they are the result of fusion process involving the capture of \(\alpha \)  particles); ii) Type Ia supernovae (SNIa), whose progenitors are generally believed to be exploding white dwarfs in binary systems, synthesise Ar, Fe and the other Fe-peak elements such as Cr and Ni, and the remaining fraction of Si and S; iii) Asymptotic giant branch (AGB) stars produce mainly C, N which are ejected through stellar winds.
